text:
ROCKY WORLDS
Zurich2024
Rocky Worlds I
Rocky Worlds II
Oxford Map
Instructions for Presenters
The poster boards are 37.5 inches (95 cm) tall and 48 inches wide (122 cm), approximately fitting A0-sized posters in landscape orientation. Printing posters locally in Oxford is possible through the Physics Media Services (pick-up in the Denys Wilkinson Building, a short walk from the conference site). Posters can stay in place throughout the week. Posters can be advertised to the entire audience by brief 1-min flash talks (see Programme). For this purpose please send a 1-slide summary to info@rockyworlds.org by 1 July. Poster flash talks will be ordered according to their arrival.
Titles & Abstracts
Pierre Auclair-Desrotour (IMCCE, Paris Observatory):
Meta-modelling the climate of synchronously rotating rocky planets
Rocky planets orbiting in the habitable zone of low-mass stars are likely to be tidally locked in 1:1 spin-orbit resonance. In this configuration, they exhibit permanent dayside and nightside, which induces a day-night temperature gradient. The resulting climate can be unstable and generate a runaway condensation of greenhouse gases on the nightside that is called atmospheric collapse. As a consequence, it is crucial to elucidate the mechanisms that govern the day-night heat redistribution on these planets to better constrain their surface conditions. In this talk, we present a hierarchical approach based on the slow rotator approximation that we call a General Circulation Meta-Model (GCMM), and that we developed as a first attempt to bridge the gap between multiple modelling approaches ranging from simplified analytical greenhouse models to sophisticated 3-D General Circulation Models (GCM). The model is able to reproduce both the closed-form solutions obtained in earlier studies, the numerical solutions obtained from GCM simulations, and solutions provided by intermediate models. We show that this approach can be efficiently used to characterise the atmospheric stability of Earth-sized rocky planets, and to disentangle the contributions of radiative transfer, atmospheric dynamics, and turbulent diffusion. Particularly, it suggests that the planetary boundary layer can play a significant role in determining the collapse pressure.
Marc Brouwers (University of Cambridge):
Prograde spin-up during gravitational collapse
Astrophysical objects on different scales appear to possess a preferential spin-orbit alignment, pointing to shared processes that tie their rotation at birth to larger parent structures. We present a new mechanism that describes how collections of particles or 'clouds' gain a prograde rotational component when they collapse or contract while subject to an external, central force. The effect is geometric in origin, as relative shear on curved orbits moves their shared center-of-mass slightly inward and toward the external potential during a collapse, exchanging orbital angular momentum into aligned (prograde) rotation. For clouds that form at the interface of shear and self-gravity, prograde spin-up means that even setups with large initial retrograde rotation collapse to form prograde-spinning objects. We highlight an application to the Solar System, where we suggest that prograde spin-up can explain the frequency of binary comets in the Kuiper belt with prograde rotation.
Ryan Boukrouche (University of Oxford):
Post-runaway climate state on rocky worlds with large water inventories
This talk will present recent results of compared 1D simulations of runaway greenhouse pure steam atmospheres, and explore ways that allows a planet to transition from the runaway greenhouse state to a post-runaway, potentially habitable climate state.
Erica Bisesi (Astronomical Observatory of Trieste - INAF):
Impact of climate on habitability of terrestrial-type exoplanets
The climate of a planet is of paramount importance to establish the possible presence of liquid water at its surface, and thus, in a wide sense generally accepted by the scientific community, its habitability. Climate depends on a high number of factors and parameters, both astrophysical (e.g., luminosity of the central star(s), distance of the planet from the star, orbital eccentricity) and planetary (inclination of the rotation axis, duration of the day, atmospheric composition and pressure, presence and fraction of oceans, presence and type of soil, orography, topography, etc.). Some of these parameters have been or will be measured in the near future; data on the others will not be available in short time, and maybe not even in the far future. Therefore simple, although approximate, climate models lend themselves to better serving at parameter space exploration (involving both well-known and unknown parameters) than the more complex Global Circulation Models (GCM), in reason of their much lower computational cost. "Simple" models allow running thousands of experiments at the same computational time of a single GCM's run. A representative example of such a streamlined model is ESTM (Earth-like Surface Temperature Model; Vladilo et al. 2013, 2015). ESTM is based on the numerical solution of a modified diffusion equation for the meridional heat transfer, coupled with a radiative-convective column atmospheric model to account for the vertical transport of radiation (downward and upward). ESTM has been used for studying a number of characteristics of possible exoplanets candidates (e.g., Silva et al. 2017). After calibration with Earth experimental data and validation with 3D climate models, ESTM has been exploited to compile more than 20,000 climate simulations of terrestrial-type planets, with the aim of understanding how variations of planetary quantities (i.e., orbital semi-major axis, eccentricity, obliquity of the rotation axis, surface geography, surface atmospheric pressure and CO2 partial pressure) not measurable with present observational techniques may affect the surface temperature and habitability of extrasolar planets (the ARTECS archive of terrestrial-type climate numerical simulations; Murante et al. 2020). Another well-known regulator of a planet's climate is its vegetation cover. Vegetation can modify the planetary surface albedo, being usually darker than the bare surface of the continents, an effect known as the "Charney mechanism" (Charney 1975, Baudena et al. 2008, Cresto Aleina et al. 2013). Here, ESTM has been exploited to investigate the impact of the Charney mechanism on an exoplanet's habitability. We are currently applying the newly developed, vegetation-switched-on version of ESTM to study the circumstellar habitable zone and exoplanets' habitability (Bisesi et al., in preparation). We are investigating how different and competing vegetation types (that resemble trees, grasslands and tree seedlings) may reach equilibrium distribution on a planet depending on its main properties (the most straightforward of these being the insolation, i.e., a combination of stellar luminosity and planet distance from the star). As different equilibrium states correspond to a different planetary surface albedo, we are estimating how vegetation can extend the planet's circumstellar habitable zone beyond its external border as a consequence of a decrease in surface albedo. In special cases known as "waterbelt" – e.g., planets almost completely covered by ice, except for a narrow band near the equator – plants could also heat up the planet, thus enlarging the liquid water band and extending the overall habitability fraction. By combing results of such simulations from the ARTECS database with the concept of GHZ (cf. Lineweaver et al. 2004; Spitoni et al. 2017) and a generalized mathematical/computational approach for estimating the probabilities of transitions and expectations for biological evolution (Bisesi and Ferluga, under submission), we finally aim at identifying which part of the Galaxy may host a fully-compatible biosphere for the development of complex life.
Andrew Buchan (Institute of Astronomy, University of Cambridge):
Planets or asteroids? How geochemistry constrains the masses of White Dwarf pollutants
Polluted white dwarfs that have accreted planetary material provide a unique opportunity to probe the interiors of exoplanetary bodies. The compositions of such bodies encode information about their formation histories, including the geological process of core-mantle differentiation, with wide ranging implications for habitability. However, the nature of the bodies which pollute white dwarfs is not well understood: are they small asteroids, minor planets, or even terrestrial planets?
In our work, we present a novel method to infer pollutant masses from detections of Ni, Cr and Si. These elements exhibit variable preference for metal and silicate during core-mantle differentiation, depending on the conditions under which it occurs. This alters their relative abundance in the core and mantle of differentiated bodies, and in turn the composition of any fragments derived from these bodies. The pressure inside the body is a key parameter, and depends on the body's mass.
By modelling core-mantle differentiation self-consistently using data from metal--silicate partitioning experiments, we place statistical constraints on the differentiation pressures (and hence masses) of bodies which pollute white dwarfs. We find 3 systems whose abundances are best explained by the accretion of fragments of small parent bodies, and 2 systems which imply accretion of fragments of Earth-sized bodies. This provides evidence for the presence of core-mantle differentiated bodies of a range of masses in exoplanetary systems.
Richard Chatterjee (University of Oxford):
Time-dependent simulation of hydrodynamic escape of planetary atmospheres
The solution of steady-state transonic planetary winds driven by stellar irradiation is a two-point boundary-value problem (BVP). The first numerical attempts used the shooting method, where the solution is found by trial-and-error and has applicability limited by its sensitivity (Watson 1981). Later, this was improved upon with the development of a relaxation method (Murray-Clay 2009) but in this you still have to guess a trial solution. It has now become clear that using an initial-value problem (IVP) approach and time-stepping the full hydrodynamic equations is the most effective solution method. The was first implemented for a terrestrial planet by Tian (2005); this was then improved on by Kuramoto (2013), and since then a range of models have been developed (e.g. Caldiroli 2021). However, not much attention has been paid to actual time evolution, either as a path to steady state or as a response to time-dependent forcing. I will present some new insights from time-dependent simulations using the CIP and CIP-CSL2 schemes (Yabe 1991, 2001); emphasising the role of viscosity in particular.
Swastik Chowbay (Indian Institute of Astrophysics):
Galactic chemical evolution of exoplanet hosting stars: Are high-mass planetary systems young?
The imprints of stellar nucleosynthesis and chemical evolution of the galaxy can be seen in different stellar populations, with older generation stars showing higher α-element abundances while the later generations becoming enriched with iron-peak elements. The evolutionary connections and chemical characteristics of circumstellar disks, stars, and their planetary companions can be inferred by studying the interdependence of planetary and host star properties. Numerous studies in the past have confirmed that high-mass giant planets are commonly found around metal-rich stars, while the stellar hosts of low-mass planets have a wide range of metallicity. In this work, we analyzed the detailed chemical abundances for a sample of >900 exoplanet hosting stars drawn from different radial velocity and transit surveys. We correlate the stellar abundance trends for α and iron-peak elements with the planets' mass. We find the planet mass-abundance correlation to be primarily negative for α-elements and marginally positive or zero for the iron-peak elements, indicating that stars hosting giant planets are relatively younger. This is further validated by the age of the host stars obtained from isochrone fitting. The later enrichment of protoplanetary material with iron and iron-peak elements is also consistent with the formation of the giant planets via the core accretion process. A higher metal fraction in the protoplanetary disk is conducive to rapid core growth, thus providing a plausible route for the formation of giant planets. This study, therefore, indicates the observed trends in stellar abundances and planet mass are most likely a natural consequence of Galactic chemical evolution.
Collin Cherubim (Harvard University):
Isotopic fractionation as a way to infer exoplanet atmospheric evolution pathways
Measurements of exoplanet radius and atmospheric isotopic fractionation offer a potential means to probe atmospheric evolution and to better constrain competing formation mechanisms. We are developing a numerical model that computes fractionation caused by atmospheric loss, with an initial focus on deuterium to hydrogen (D/H) enhancement on sub-Neptunes. Using mass-radius relations derived from thermal evolution models, we postdict initial atmospheric mass fraction and isotope enhancement by comparing present-day radius estimates to model predictions based on a specified escape pathway. Our preliminary results suggest that the degree of fractionation is sensitive to both the type of escape process and the planet's initial H2 inventory. We are currently investigating the degree to which various fractionation patterns can be constrained from transmission spectroscopy.
Jessica Cmiel (Harvard University): Volatile Partitioning on Early Venus
Magma oceans play a crucial role in establishing the initial conditions for different evolutionary paths of terrestrial planet atmospheres. The speciation of volatiles between a planet's magma ocean and atmosphere is dependent on effects such as chemical solubility and redox state, as characterized by the oxygen fugacity (ƒO2) of the magma. This in turn has important implications for an emerging planet's atmospheric composition. We are developing a new coupled model that incorporates volatile partitioning and oxygen fugacity changes in a terrestrial planet with a magma ocean. We are using this model to to understand how hydrodynamic H escape and other redox-varying processes influenced the chemical partitioning of volatile species on early Venus. Our ultimate aim is to constrain the range of possible initial atmospheric compositions on Venus to understand how its early climate may have evolved relative to Earth's.
Alfred Curry (Imperial College London):
Investigating rocky interiors by modelling disintegrating exoplanets
Vera Dobos (Kapteyn Astronomical Institute, University of Groningen):
A target list for searching habitable exomoons
Although there are no confirmed exomoon discoveries to date, their potential habitability is an important question. Extending the search for life to exomoons expands our possibilities and chances to find habitable environments outside the Solar System. Detecting the first habitable exomoon will provide great opportunities to study and characterize this new type of extra-solar body. In this talk I will present our latest work which provides a target list for observing exoplanets which can host large, habitable moons on stable orbits. To determine their habitability, we calculated the incident stellar radiation and the tidal heating flux arising in the moons as the two main contributors to the energy budget. We used the runaway greenhouse and the maximum greenhouse flux limits as a definition of habitability. For each exoplanet we ran our calculations for plausible ranges of physical and orbital parameters for the moons and the planet using a Monte Carlo approach. Two promising candidates in our list are Kepler-62 f and Kepler-16 b, both of them with known masses and radii. Our target list can help to detect the first habitable exomoon.
Jingyao Dou (University of Bristol):
Giant impact benchmark tests between GADGET2 and SWIFT
Smoothed Particle Hydrodynamics (SPH) is a Lagrangian particle-based method that has been widely used to study giant impacts, where planets are modelled with particles that evolve under gravity and material pressure. SWIFT is a recently developed hydrodynamics and gravity code for astrophysics and cosmology which can be used as a drop-in replacement for GADGET-2 and is reported to have a faster runtime on representative cosmological problems. We compared the performance and results of the two codes in terms of planetary giant impact simulations and found that the run time and simulation results of SWIFT will greatly depend on the maximum smoothing length set in the code. Given proper maximum smoothing length, SWIFT could run giant impact simulations faster than that of the GADGET-2 while the final results of the two codes were similar. We are currently using SWIFT to study the erosion of a protoplanet's atmosphere during a giant impact when there is an ocean at the surface of the planet.
Vanessa Emeka-Okafor (University of Warwick)
Namrah Habib (University of Oxford):
Modelling Dry Compositional Convection for Applications to Terrestrial Exoplanets
Mark Hammond (University of Oxford):
The Overturning Circulation and Day-Night Temperature Contrast on Tidally Locked Rocky Planets
Tidally locked planets always present the same side to their host star. The difference in temperature between their permanent day-side and permanent night-side is a key contributor to their habitability and atmospheric stability. It also plays a key role in observations of atmospheric composition and temperature structure. We show that on a planet with an atmosphere, this temperature difference is almost entirely governed by one component of the atmospheric circulation -- the overturning circulation. We derive a predictive model of this circulation and compare its predicted day-night temperature contrast to simulations in 3D atmospheric models.
Dongyang Huang (ETH Zurich):
Nitrogen speciation in a terrestrial magma ocean and an N-enriched secondary atmosphere
Rolf Kuiper (University of Duisburg-Essen):
The Recycling Hypothesis in the Formation of Proto-planet's first Atmospheres
In the core accretion paradigm of planet formation, gas giants form a massive atmosphere in a run-away gas accretion phase once their progenitors exceed a threshold mass: the critical core mass. On the one hand, the majority of observed exo-planets, being smaller and rock/ice-dominated, never crossed this line. On the other hand, these exo-planets have accreted substantial amounts of gas from the circumstellar disk during their embedded formation epoch.
We investigate the hydrodynamical and thermodynamical properties of proto-planetary atmospheres by direct numerical modeling of their formation epoch. Our studies cover one-dimensional (1D) spherically symmetric, two-dimensional (2D) axially symmetric, and three-dimensional (3D) hydrodynamical simulations with and without radiation transport. We check the feasibility of different numerical grid geometries (Cartesian vs. spherical), perform convergence studies, and scan the physical parameter space with respect to planet mass and optical depth of the surrounding.
In terms of hydrodynamic evolution, no clear boundary demarcates bound atmospheric gas from disk material in a 3D scenario in contrast to 1D and 2D computations. Atmospheres denote open systems where gas enters and leaves the Bondi /Hill sphere in both directions. In terms of thermodynamics, we compare the gravitational contraction of the forming atmospheres with its radiative cooling and hydrodynamical advection of energy, as well as the interplay of these processes. The coaction of radiative cooling of atmospheric gas and advection of atmospheric-disk gas prevents the proto-planets to undergo run-away gas accretion. Hence, this recycling process provides a natural explanation for the preponderance of super-Earth like planets.
To advertise the general purpose approach of our code development, I will also briefly overview the most recent results obtained in a variety of other astrophysical research fields from proto-planets on supersonic, eccentric orbits (Mai et al. 2020), to accretion and multiplicity in massive star formation (Oliva & Kuiper 2020), up to the formation of the progenitors of the first supermassive black holes in the early universe (Hirano et al. 2017, Science).
Matt Lodge (University of Bristol):
Scattering from Non-Spherical Aerosol Aggregates in Exoplanet Atmospheres
The majority of atmospheric scattering models assume spherical particles to allow fast computation of their optical parameters. However, evidence from atmospheric studies on Earth suggests particles often display more complex geometries, for example exhibiting fractal structures with distinct monomers. This research aims to explore the consequences on the optical properties of non-spherical aerosols, and in particular, the consequences for modelling the transmission spectra of exoplanet atmospheres.
Erik Meier (Center for Space and Habitability, University of Bern):
Variable occultation depth of 55 Cnc e in the visible range
Among the numerous super-Earths discovered so far, 55 Cnc e presents itself as one of the most mysterious exoplanets. It has been observed that the occultation depth of the planet, with an orbital period of 0.73 days, changes significantly over time at mid-infrared wavelengths. Observations with Spitzer measured a change in its day-side brightness temperature of 1200 K, possibly driven by volcanic activity, magnetic star-planet interaction, or the presence of a circumstellar torus of dust. Here we present that the variability exists also in the optical.
TESS observed 55 Cnc during sectors 21, 44 and 46. We report an occultation depth of 8±2.5 ppm for the complete set of TESS observations. In particular, we measured a depth of 15±4 ppm for sector 21, while for sector 44 we detect no occultation. In sector 46 we measure a weak occultation of 8±5 ppm. The occultation depth varies from one sector to the next between 1.6 and 3.4 σ significance. We also derived the possible contribution on reflected light and thermal emission, setting an upper limit on the geometric albedo.
Based on a model comparison between varying occultation across sectors, a constant occultation and no occultation at all, the presence of an occultation is favoured considerably over no occultation, where the model with varying occultation across sectors takes most of the statistical weight.
Our analysis confirms a detection of the occultation in TESS. Moreover, our results weakly lean towards a varying occultation depth between each sector. The process responsible for this phenomenon is still unknown, but future missions, such as JWST, might provide the key pieces to this puzzling system.
Juliana García-Mejía (Harvard University):
First Light Results from the Tierras Observatory, An Ultra-precise Time-series M-dwarf Photometer
We are engaged in a project to refashion the 1.3m 2MASS telescope located at the F.L. Whipple Observatory atop Mount Hopkins, Arizona, into an ultra-precise time-series photometer: The Tierras Observatory is designed to achieve a photometric precision of 250 ppm across an observing season. The design choices that enable this precision include a four-lens focal reducer and field-flattener to increase the field-of-view of the telescope from 12 arc minutes to 0.48 degrees on a side; a custom narrow (40 nm) bandpass filter centered around 863.5 nm to minimize precipitable water vapor errors known to limit ground-based photometry of M dwarfs; a deep-depletion 4k x 4k CCD with a quantum efficiency of 85% in our bandpass, operating in frame transfer mode; and, a fully automated observing mode. Tierras achieved first light in the fall of 2021, and in February 2022 we installed a new set of baffles to significantly reduce sky background. We will share recent light curves and summarize our current on-sky performance. Tierras is starting a three-year survey of M dwarf stars within 15 parsecs to detect new terrestrial planets that were too small or too cool to be found by TESS or previous ground-based efforts, and to monitor known exoplanets (both rocky and gaseous) to search for satellites or systems of circumstellar rings. Furthermore, a long term monitoring campaign will permit Tierras to determine M dwarf rotation periods, elucidating the process and timescale over which these stars lose their angular momentum.
Claire Guimond (University of Cambridge):
Limits to land planets, and how to store oceans on or inside them
Do we expect many rocky planets to have both oceans and dry land? Directly detecting exoplanet surfaces will be at the least extremely difficult, yet this information is key to interpreting climate models and biosignatures. Whilst Earth's marbled appearance seems to have emerged from complex, entwined systems, one imagines multiple ways to create the same effect on planets in different geodynamic regimes. We take first steps towards estimating the frequency of extrasolar blue marbles by modelling the simplest processes that set planetary land/ocean fractions. On one hand, topography increases land propensity by hollowing out ocean basins, storing surface water. To this end we quantify how dynamic topography---surface undulations caused by upwelling mantle---scales with constrainable bulk planet properties. Such scalings can tell us the minimum (pessimistic) ocean mass that would flood a planet. On the other hand, a higher total water budget will push a planet towards a fully water-covered regime. We expect planetary mantles to be a large reservoir for water (i.e., hydrogen stored in minerals), which over time supplies the surface via outgassing. Thus we also preliminarily estimate maximum mantle water capacities as a function of stellar-derived mineralogy. Together, limits on topography and on water budgets present two uses of deterministic geophysical modelling towards understanding aspects of rocky worlds not accessible to observation.
Sean Jordan (Institute of Astronomy, University of Cambridge):
Metabolic Signatures of an Aerial Biosphere in the Clouds of Venus
Life in the clouds of Venus, if present in sufficiently high abundance, must be affecting the atmospheric chemistry. It has been proposed that abundant Venusian life could obtain energy from its environment using three possible sulfur-based metabolisms. These metabolisms raise the possibility of Venus's enigmatic cloud-layer SO2-depletion being caused by life. We couple each metabolic pathway to a photochemical-kinetics model and self-consistently predict the composition of Venus's atmosphere under the scenario that life produces the observed SO2-depletion. Using this photo-bio-chemical kinetics model, we show that all three metabolisms can produce SO2-depletions, but do so by violating other observational constraints on Venus's atmospheric chemistry. We calculate the maximum possible biomass density of sulfur-metabolising life in the clouds, before violating observational constraints, to be ~ 10^-5 - 10^-3 mg m-3. The methods employed are equally applicable to aerial biospheres on Venus-like exoplanets, planets that are optimally poised for atmospheric characterisation in the near future.
Giuseppe Murante (INAF-Trieste Observatory):
Climate bistability of Earth-like exoplanets
Before about 500 million years ago, most probably our planet experienced temporary snowball conditions, with continental and sea ices covering a large fraction of its surface. This points to a potential bistability of Earth's climate that can have at least two different (statistical) equilibrium states for the same external forcing (I.e. solar radiation). Here, I will explore the probability of finding bistable climates in Earth-like exoplanets and consider the properties of planetary climates obtained by varying the semimajor orbital axis (thus, received stellar radiation), eccentricity and obliquity, and atmospheric pressure. To this goal, we used the Earth-like planet surface temperature model (ESTM), an extension of one-dimensional Energy Balance Models developed to provide a numerically efficient climate estimator for parameter sensitivity studies and long climatic simulations. I will shortly describe out model. After verifying that the ESTM is able to reproduce Earth climate bistability, we identify the range of parameter space where climate bistability is detected. An intriguing result of this work is that the planetary conditions that support climate bistability are remarkably similar to those required for the sustenance of complex, multicellular life on the planetary surface. The interpretation of this result deserves further investigation, given its relevance for the potential distribution of life in exoplanetary systems.
Claire Nichols (Department of Earth Sciences, University of Oxford):
A Time-Resolved Paleomagnetic Record of Main Group Pallasites: Evidence for a Large-Cored, Thin-Mantled Parent Body
Several paleomagnetic studies have been conducted on five Main Group pallasites: Brenham, Marjalahti, Springwater, Imilac, and Esquel. These pallasites have distinct cooling histories, meaning that their paleomagnetic records may have been acquired at different times during the thermal evolution of their parent body. Here, we compile new and existing data to present the most complete time- resolved paleomagnetic record for a planetesimal, which includes a period of quiescence prior to core solidification as well as dynamo activity generated by compositional convection during core solidification. We present new paleomagnetic data for the Springwater pallasite, which constrains the timing of core solidification. Our results suggest that in order to generate the observed strong paleointensities (∼65–95 μT), the pallasites must have been relatively close to the dynamo source. Our thermal and dynamo models predict that the Main Group pallasites originate from a planetesimal with a large core (>200 km) and a thin mantle (<70 km).
Anjali Piette (Carnegie Earth & Planets Laboratory):
Atmospheric Retrieval of Rocky Exoplanets in Thermal Emission
Emission spectroscopy is a promising technique to observe atmospheres of rocky exoplanets, probing both their chemistry and thermal profiles. I will present HyDRo, an atmospheric retrieval framework for thermal emission spectra of rocky exoplanets. HyDRo does not make prior assumptions about the background atmospheric composition, and can therefore be used to interpret spectra of secondary atmospheres with unknown compositions. I will further show how HyDRo can be used to assess the chemical constraints which can be placed on rocky exoplanet atmospheres using JWST. I identify the best currently-known rocky exoplanet candidates for spectroscopic observations in thermal emission with JWST, finding >30 known planets whose thermal emission will be detectable by JWST/MIRI in fewer than 10 eclipses at R~10. I then consider the observations required to characterise the atmospheres of three promising rocky exoplanets across the ~400-800K equilibrium temperature range: Trappist-1b, GJ1132b, and LHS3844b. Considering a range of CO2- to H2O-rich atmospheric compositions, I find that CO2 and H2O can be detected in these atmospheres with reasonable amounts of JWST observing time, and that their abundances can be constrained with good precision. Finally, I will discuss the impact of clouds on emission spectra of rocky exoplanets and on their atmospheric retrievals. HyDRo will allow important atmospheric constraints on rocky exoplanets with JWST observations, providing crucial insights into their geochemical environments.
David Rice (University of Nevada, Las Vegas):
Investigating systematic uncertainties in terrestrial interior models with MAGRATHEA
The community uses a variety of models to characterize the interior structure of small planets. Underlying these models are multiple computational techniques, numerous experimental measurements and theoretical estimates of the equations of state for planet-building materials, and differing treatments of temperature. MAGRATHEA is an open-source interior structure solver which can be customized to user-defined planet models. Our code features adaptable phase diagrams for the core, mantle, hydrosphere, and atmosphere and transparent storage for equations of state. I will demonstrate how the community can use and contribute to the code. I then use MAGRATHEA to test model parameters and quantify systematic uncertainties in the characterization of small planets such as those in the Trappist-1, K2-138, and K2-146 systems.
Robert Ridgway (University of Exeter):
3D Modelling of the Impact of Stellar Flares on Earth-like Rocky Planets Orbiting M Dwarf Stars
The current best candidates for habitable exoplanets have been detected orbiting M-dwarf stars. Such stars are quite common, and their low brightness and the short orbital periods of their planets both aid observations. Many M dwarf stars are known to produce stellar flares, phenomena where the star releases substantial amounts of energy, particularly in the ultraviolet (UV) and becomes much brighter for a period of minutes to hours. In addition, flares are associated with a release of energetic protons from the star, known as stellar proton events. Flares released by the Sun are less energetic than those of M dwarfs. This presents some questions about the habitability of exoplanets around M dwarfs. The increased UV light and the protons may induce long-term changes in the exoplanetary atmosphere by destroying molecules such as ozone that help shield the surface from the UV. This would make the planet's surface dangerous for terrestrial life and may make the emergence and survival of surface-based life impossible. I present results from a study in 3D using the UK Met Office global circulation model, termed the Unified Model (UM). The UM has been adapted to model a wide range of exoplanets. I present the results from simulations including a coupled chemical kinetics and photolysis scheme. Our chemical network describes the production of ozone via the Chapman cycle as well as the change in ozone due to HOx and NOx photochemistry. A tidally locked aquaplanet with an Earth-like atmosphere is simulated for twenty years under quiescent conditions before it is subjected to a series of flares of varying total energies drawn from a realistic distribution. I will describe the changes in the atmospheric composition as well as surface habitability that occur due to the flares.
Suman Saha (Indian Institute of Astrophysics):
Detection and Characterization of Habitable Exomoons
Rocky exomoons in the habitable zones of the exoplanetary systems hold special significance as they can host life. Although the detection of exomoons has yet remained elusive, mainly due to their smaller expected size, the next generation space missions such as JWST can provide unique opportunity for such detection. In this talk, I will present a comprehensive analytical formalism in order to model the lightcurves of transiting exoplanets hosting exomoons. In order to achieve an analytical formalism, we have considered circular orbit for the exomoon around the host planet, which is indeed the case for tidally locked moons. The formalism takes care of the co-alignement or non-coalignment of the orbits of the planet and the moon using a two angular parameter approach and can be used to model and characterize all the possible orbital alignments for a star-planet-moon system. Using this formulation, we have studied the detectability of rocky exomoons using next generation telescopes, such as JWST. We have also studied the observational limits on the characterization of the atmospheres of such exomoons using JWST.
Joseph Schulze (Ohio State University):
Uncertain planets: determining how precisely we can know rocky planet composition given equation of state limitations
The most fundamental inputs of rocky planet structure models, used to build mass-radius relationships and infer composition, are the underlying material-dependent equations of state (EOS) of core and mantle minerals. Such models often assume idealized compositions, neglect EOS uncertainties when extrapolating, and ignore EOS-to-EOS discrepancies, or use EsOS based on biased data. Separately, these effects can lead to model-dependent planet densities that vary by 1-10% over the observed rocky planet mass range. Several probable rocky planets now have density characterization to better than or near 10% uncertainty, meaning we are we are fast approaching an era where EOS uncertainty and variability must be carefully considered. Failing to do so will yield erroneously precise compositions which, in turn, may over-constrain planet formation/evolution models. Here, I quantify how precisely we can know super-Earth interiors given EOS uncertainty/variability and make material-specific EOS recommendations based on best practices in mineral physics. I combine my results with observational uncertainties into an open-source structure model for calculating the exact compositional uncertainties of rocky planets.
Marie-Luise Steinmeyer (GLOBE Institute, University of Copenhagen):
Envelopes around rocky planets during pebble accretion
The process of pebble accretion forms planets during the lifetime of the protoplanetary disks. These protoplanets are thus able to acquire gas envelopes during their growth period. Due to accretion heating, the temperature in the envelope can become high for pebbles to sublimate before they reach the embryo. At the same time, there exist recycling gas flows between the planetary envelope and the surrounding disk. Understanding the evolution of the gas envelopes and the sublimated pebbles is therefore key to understanding the composition protoplanet.
I present nested-grid, high-resolution 3D hydrodynamic simulations of pebble accretion on rocky protoplanets using the Dispatch framework (Nordlund et al., 2018; Popovas et al., 2018). The simulations extend down to the planetary surface. Therefore, my work is able to resolve the gas motion close a protoplanet during pebble accretion. I introduced gas tracers to the setup in order to study this motion in more detail. In addition, I present 1D models of these envelopes around low mass protoplanets to study the location of the sublimation fronts of different solids.
In the adiabatic limit, the recycling flow penetrates the Hill sphere of rocky protoplanets. Inside the Bondi sphere, the gas is bound to the planet. The 1D models including radiative transfer show a two-layer envelope with an inner convective and an outer radiative region. The sublimation fronts are located deep in convection region of the protoplanets.
Christiaan Van Buchem (Leiden University):
Modeling silicate atmospheres on hot rocky exoplanets
Hot rocky exoplanets with equilibrium temperatures above ∼2000 K (e.g. 55 Cnc e, K2-141 b, and GJ 367 b) are thought that have molten surfaces. This implies that there is a direct interface between the planet's lava ocean and atmosphere. Hence, the composition of these planet's atmospheres is likely to be closely linked to the composition of their lava oceans. This provides a unique opportunity for astronomers to characterize the mantle composition of such planets based on the composition of their atmospheres. With the recent launch of JWST and the future prospect of ARIEL ushering in a new era of exoplanet observations, this topic is now more relevant than ever.
In order to accomplish this, we must first gain a deeper understanding of the way in which a lava ocean interacts with an atmosphere. The first step in this process is to model the outgassing that takes place in a silicate melt. Using the thermodynamic data of the magma ocean provided by the MELTS code, we developed an open source code that predicts the composition of such a vaporised atmosphere for a given magma composition and temperature. In this poster we will present out methods, results, validation with lab data, and comparison to other similar codes.
The successful development of this method and subsequent comparisons to observations would allow us to start characterising rocky exoplanet compositions based on their atmo- sphere compositions, which could lead to new insights for formation models. Furthermore, it would also allow us to model the effects of transient magma oceans though to be present on young earth analogs. Deepening our understanding of how such processes influence the conditions present during later evolutionary stages and possibly give us new insights in the conditions necessary to sustain life.
Iris van Zelst (Institute of Planetary Research, German Aerospace Center):
Towards interior-atmosphere coupling on Venus
The evolution of the atmospheric composition of a planet is largely determined by the partial melting and volcanic outgassing of the interior. In turn, the composition of the atmosphere dictates the surface temperature of the planet (due to processes like the greenhouse effect), which is an important boundary condition for crustal and mantle processes in the interior of a planet. Venus in particular has a large atmosphere with an abundance of the greenhouse gas CO2 and a small amount of water vapour, which can significantly change the surface temperature and hence global mantle evolution of Venus. Since much of Venus' evolution still remains elusive, we aim to study the coupled interior-atmosphere evolution of Venus to shed new light on Earth's twin.
Here, we show the first results of coupling a grey atmosphere model (i.e., we assume that the absorption coefficients are constant and hence independent of frequency) considering only CO2 and H2O as greenhouse gases to the geodynamic code Gaia. We compare to previous studies who employed similar coupled models (e.g., Noack et al., 2012; Gillmann & Tackley, 2014; Höning et al., 2021). We also speculate how we could further expand the coupled atmospheric model to account for other chemical species such as sulfur and nitrogen.
Andrew Walker (Department of Earth Sciences, University of Oxford):
Non-equilibrium snow zones in planetary cores built from growing and sinking iron crystals
We describe a model of the formation of iron snow zones in planetary cores which have implications for the long timescale thermal evolution of planets and on the generation of an internal magnetic field. These two-phase snow zones are composed of a mixture of light-element enriched liquid and a small fraction of solid iron crystals. In contrast to most previous descriptions, we focus on modelling the physics controlling the growth and sinking of individual iron crystals and do not assume that the snow layer is in phase equilibrium. This means that our model does not require the temperature and solid volume to be linked through a liquidus relation and yields a distribution of solid grain sizes throughout the layer.
We consider the layer as a liquid iron-oxygen alloy cooled below the liquidus temperature such that microscopic solid iron crystals can form. Each crystal sinks because it is denser than the surrounding liquid. As the crystal sinks it also grows because of the chemical potential difference between iron in the solid and liquid phases. Growing crystals reject oxygen, moving the system towards equilibrium, but this equilibration is limited by the intrinsic growth kinetics of iron and by the need for iron to diffuse through an oxygen enriched boundary layer around the falling crystal. We model the layer as a collection of independently falling crystals which form throughout the layer and only interact by changing the composition of the liquid. Assuming the layer is in steady state and imposing the crystal formation rate, the temperature, and the overall composition, allows us to solve for the volume fraction of solid in the layer, the composition of the liquid, the size distribution of crystals, and, for deep snow zones, the growth rate of the planet's inner core.


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Lafayette Considers Expansion, One Nearby Town Strikes Itself From List
Wed, March 25, 2015 | Posted by Lisa Gonzalez
We have long applauded communities that have built their own fiber networks and then elect to expand them to neighboring communities. In Louisiana for example, Lafayette could hoard its network, forcing people that want the best connectivity in the region to move within its borders. But instead, it is preparing to expand the network.
City-Parish President Joey Durel announced that the municipal network would begin expanding beyond Lafayette city limits. An article in The Advocate quoted Durel:
"As I have traveled this parish, one of the most common things I am asked is, 'When will we get fiber?' That answer depended in large part on making fiber successful in Lafayette. We're there," Durel told the crowd that filled the Cajundome Convention Center.
Durel noted that municipalities that make agreements with Lafayette based on future annexation will be considered if they are willing to pay for the cost of expansion in their communities. Youngsville is reported to be the first town be consider Lafayette's proposal for bringing better local residential and business connectivity.
Any expansion of municipal networks has to answer some of the same important questions of any partnerships - how to allocate risk and benefits. It doesn't seem appropriate for Lafayette to assume the full risk of expanding the network to Youngsville, for example. Those who receive the benefits should assume some risk, and those who assume risk should be compensated in some measure.
One community, Broussard, is balking. Apparently, the town of 6,800 people located just outside Lafayette city limits does not want to contribute to the cost of fiber in their community, reports The Advocate. Understanding these fights from afar is always challenging because neighboring communities have often developed animosity over decades from both real and imagined slights.
Broussard has taken a hard line:
"There is no way we are going to give LUS the money to extend their fiber lines in Broussard for them to profit off of our infrastructure and the business of our citizens," Broussard Councilman and Mayor Pro-Tem Johnnie Foco said in a statement…
Seeing such strong statements, we are forced to recall the extremes Cox Cable has gone to in an effort to thwart potential competition in the past. We don't know the terms LUS is offering, though we hope to update our reporting on this in coming days. What we do know is that expanding the LUS Fiber network will require a significant capital cost and risk. If Broussard doesn't want to contribute it all, it should get used to its Cox monopoly.
joey durel
LUS Fiber "Ask Me Anything" July 14th 1:30 p.m. CDT
Lafayette Celebrates 10 Year Anniversary of "Yes" to Network
LUS Fiber Leaders Have Sit-Down With Discover Lafayette: Watch and Learn
Opportunities and Challenges as Lafayette Considers Muni Fiber Expansion - Community Broadband Bits Episode 144
LUS Fiber Expanding To Two Neighboring Communities
"Municipal broadband may or may not make sense for a particular community, but the idea is not exactly one being pushed by beret-capped socialists quoting "Das Kapital." On the contrary, it's cold-eyed disciples of Adam Smith — specifically business leaders, the captains of the private sector — who are usually the most enthusiastic champions."

redpajama_set_name: RedPajamaCommonCrawl


Evaluate This Site I Have - Potential Gold Mine?
Discussion in 'Site Flipping' started by Smokin, Apr 15, 2013.
Anyways, about the site, it's an Article site..
I just recently started averaging $5/day on AdSense.. I know I could monetize this way more with the traffic I am getting, which is a reason why I would to sell as well (more value?).
Several of the posts are #1 search return on google, receiving several hundred uniques, EACH per month.
Of this the userbase contains 35k emails which are unmarketed.
How much is something like this worth to the right buyer and how much would an e-mail like this be worth?
Please advise, and good feedback (positive or negative) will receive +rep.
Thank you for all of the knowledge BHW!!
1.87 million views, and a 35k email list, i wouldn't be selling that to anyone. You must be able to figure out how to make more than a $5 a day though, that is terrible!
After i looked your site it's seems to be a "SPAM PLACE" the traffic you are getting is 70-80% seems to be spammy bots which comes to your site to submit article with their backlink for seo purpose only.
My evaluation says it's worth less than $100.
Traffic is questionable at best. Probably why it doesn't convert.
The website design isn't creative or appealing. Nothing to work with there that can't be done in 20 minutes.
The email list is most likely all fake emails used by spammers submitting articles to directories.
The PR2 you claimed is PR1 today.
The backlink profile is terrible. Surprised the site hasn't suffered a penalty yet. I'm sure its days are numbered. One of the few domains I've seen where the fresh index is worst than the historical index.
Once you get an Alexa ranking under 100K we can dig deep into your traffic and it doesn't look good at all.
Good luck with your offers but IMO I don't see much value at all here.
I will give you 100 dollars.
You get bot traffic. Not human traffic. That is why your adsense is so low.


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Alta (en sami septentrional: Áltá; en finès: Alattio) és una ciutat i municipi del comtat de Troms og Finnmark, Noruega. Té una població de 19.822 habitants (2014) i ocupa una superfície de 3.849,42 km².

Limita al nord amb Hasvik, Hammerfest, Loppa i Kvalsund; al sud amb Porsáŋgu, a l'est amb Guovdageaidnu i Kárášjohka, i a l'oest amb Kvænangen i Loppa.

És el principal centre de comunicacions de Finnmark i, malgrat no ser la capital del comtat, és la ciutat més important i amb més població. Les aigües que banyen la costa del municipi estan cobertes de salmó, que és el motor principal de l'economia a la ciutat.
Destaca l'Art rupestre d'Alta format per un conjunt de petròglifs declarats Patrimoni de la Humanitat.

Informació general

Etimologia
El nom del municipi prové del local fiord d'Alta. El topònim prové del nòrdic antic ǫlpt, que fa referència a un cigne o és una norueguització de la paraula finlandesa alaattia, que fa referència a una 'terra baixa'. Abans del 1918, el nom era escrit Alten.

Escut d'armes
L'escut d'armes és de temps moderns (1976). Mostra la punta d'una fletxa, en referència a les puntes de fletxes de quars (que daten del paleolític), trobades a la ciutat.

Geografia
El municipi té una extensió 3.845 km² a l'oest del comtat, principalment al llarg del fiord d'Alta. És cobert amb grans masses forestals i ocupa una part de l'altiplà de Finnmarksvidda. El riu Áltá ha format un dels més grans canyons d'Europa, al seu curs des de l'altiplà fins al fons.

Alta es troba a la Noruega continental, això no obstant també inclou algunes petites illes. Seiland és la llar del Parc Nacional Seiland, on s'hi troba la glacera Seilandsjøkelen i la muntanya Seilandstuva. El parc també inclou centenars de llacs.

Clima
La majoria de la població viu al llarg de l'interior del fiord, on gaudeix d'un clima protegit subàrtic, on les temperatures mitjanes diàries estan per sobre de 10 graus centígrads tan sols 3 mesos l'any. Les temperatures diürnes mitjanes d'estiu solen ser comparables amb zones del sud de Noruega, i les terres baixes d'Alta estan protegides majoritàriament de les tempestes de l'hivern. La temperatura mitjana anual és d'1,3 °C. La vall d'Alta està dominada per boscos bedoll i pi roig. La precipitació és baixa, amb una mitjana anual de tan sols 420 mil·límetres. Els cels clars són la raó per la qual Alta és escollida com una localització excel·lent per a estudiar l'aurora boreal.

Història

Els dibuixos sobre la roca d'Alta, que daten del vora el 4200 aC fins al 500 aC, han estat declarats Patrimoni de la Humanitat per la UNESCO. A més, la cultura Komsa es diu així precisament per la muntanya del mateix nom del municipi d'Áltá, on es van descobrir les primeres restes arqueològiques.

Els residents kvens d'Alta són en gran part descendents dels immigrants finlandesos que van arribar a la regió ja abans del .

En la Segona Guerra mundial, el cuirassat alemany Tirpitz utilitzava l'Altafjord com a port, i el van destruir amb atacs aeris els aliats.

La controvèrsia d'Alta va provocar molts titulars durant setmanes el 1979, ja que molta gent (especialment grups ecologistes) volien evitar l'edificació d'una presa per produir electricitat, amb manifestacions i formes de desobediència civil. La presa es construí, tanmateix, i el riu encara ofereix bona pesca de salmó.

Alta es convertia en ciutat el 1999. La població ha anat creixent de manera constant.

Comunicacions i economia

Alta és un centre de comunicacions a Finnmark. Per l'aeroport d'Alta, hi van passar 308.000 passatgers el 2004. Hi ha vols directes a Oslo. Alta també té un port al centre de la ciutat i és travessada per la carretera E6, la principal via de comunicació entre el nord i el sud de Noruega.

Les activitats principals a Alta inclouen el comerç, la petita indústria, l'educació i els serveis. La ciutat és també famosa per la seva indústria de pissarra. La Universitat de Finnmark (Høgskolen Finnmark) es troba a Alta, i hi ha també un institut d'investigació (Norut NIBR Finnmark). La ciutat té l'hotel de gel situat més al nord d'Europa.

La ciutat és una de les que estan a més quilòmetres de la capital del país, d'Oslo.

Ciutats agermanades
Alta manté una relació d'agermanament amb les localitats següents:
  Apatitt, província de Múrmansk, Rússia
  Boden, comtat de Norrbotten, Suècia
  Oulu, Ostrobòtnia del Nord, Finlàndia (des de 1948)

Vegeu també
 Museu d'Alta
 Catedral de les Llums del Nord

Referències

Patrimoni de la Humanitat a Noruega
Entitats de població de Troms og Finnmark
Municipis de Troms og Finnmark

redpajama_set_name: RedPajamaWikipedia


Please join us at Nashville's own Parnassus Books in Green Hills for the release of our third guidebook in the Little Roads Europe Travel Guides series. Our newest guide explores the back roads of Ireland: We seek out the evocative ruins of medieval and prehistoric sites; we find little-known alternatives to the big tourist attractions and most famous landscapes; and of course we discover rich sources of excellent food prepared with skill and love by the charming people of Ireland.
Our book event at Parnassus will feature tastes of Irish stout beer and homemade Irish soda bread (with Irish butter of course!). Come for a bite, a fun read, and "good craic!"


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Insight News November 6, 2020 Business, Leadership, U.S., Uncategorized
In Torrent of Falsehoods, Trump Claims Election Is Being Stolen
It was an alternate version of reality, one in which Donald Trump was not losing but the victim of a wide-ranging conspiracy stretching across the country in multiple cities, counties and states, involving untold numbers of people all somehow collaborating to steal the election in ways he could not actually explain.
Never mind that Mr. Trump presented not a shred of evidence during his first public appearance since late on election night or that few senior Republican officeholders endorsed his false claims of far-reaching fraud. A presidency born in a lie about Barack Obama's birthplace appeared on the edge of ending in a lie about his own faltering bid for re-election.
"If you count the legal votes, I easily win," Mr. Trump said Thursday night in an unusually subdued, 17-minute televised statement from the lectern in the White House briefing room, complaining that Democrats, the news media, pollsters, big technology companies and nonpartisan election workers had all corruptly sought to deny him a second term.
"This is a case where they're trying to steal an election," he said. "They're trying to rig an election, and we can't let that happen."
He convinced few people who were not already in his corner. Most of the television networks cut away from the statement on the grounds that what Mr. Trump was saying was not true.
On CNN, former Senator Rick Santorum of Pennsylvania, a Republican often put in the position of defending Mr. Trump over the years, appeared exasperated as he denounced the president's loose talk of election thievery as "dangerous" and "shocking" and declared that "counting absentee ballots and counting mail-in ballots is not fraud."
The New York Post, which published salacious articles on Hunter Biden planted by Mr. Trump's associates before the election, headlined an article: "Downcast Trump Makes Baseless Election Fraud Claims in White House Address."
Even Fox News noted it had seen no "hard evidence" of widespread wrongdoing, although it later reversed its position and instructed to not refer to Mr. Biden as "President Elect" and its hosts, including Sean Hannity, went on a tyrant, accusing the nation of "stealing" the election from his friend, Donald.
"There is no defense for the President's comments tonight undermining our Democratic process," Gov. Larry Hogan, Republican of Maryland and a critic of the president, wrote on Twitter. "America is counting the votes, and we must respect the results as we always have before. No election or person is more important than our Democracy."
Former Gov. Chris Christie, Republican of New Jersey and a longtime ally of Mr. Trump's, likewise disputed the president. "I talk tonight now not as a former governor but as a former U.S. attorney — there's just no basis to make that argument tonight," he said on ABC News. "There just isn't."
With his presidency on the line, Mr. Trump's lonely appearance in the briefing room with no allies joining him and only staff members and reporters in attendance underscored how isolated he has become just two days after Election Day. With vote counts in key states turning grimmer even as he spoke, Mr. Trump was poised to end this term in office the way he began his presidential campaign in 2015 — defended most vocally by family members and a few loyalists while Republican leaders held him at arm's length rather than embrace outlandish claims.
However, Trump has picked up some support from fellow Republicans. After Donald Trump Jr. went after Senator Lindsey Graham, Republican of South Carolina, for not speaking up, the senator went on Sean Hannity's show on Fox on Thursday night and came to the president's defense. The Senate Judiciary Chairman told Hannity Thursday he will donate $500,000 to the Trump campaign's legal efforts to challenge election procedures in multiple states, including Pennsylvania, Michigan and Nevada.
Discussing the ongoing ballot counting in Philadelphia that has shrunk the president's lead over Democrat Joe Biden, Graham described elections in the City of Brotherly Love as being "crooked as a snake."
Members of Mr. Trump's inner circle sounded almost desperate as they sought to threaten other Republicans into backing Mr. Trump. Both Donald Trump Jr. and Eric Trump posted messages on Twitter complaining that Republicans were not standing with their father, especially those who may want his support if they run for president in four years.
"The total lack of action from virtually all of the '2024 GOP hopefuls' is pretty amazing," Donald Trump Jr. wrote. "They have a perfect platform to show that they're willing & able to fight but they will cower to the media mob instead."
"Where are Republicans!" Eric Trump added about an hour and a half later. "Have some backbone. Fight against this fraud. Our voters will never forget you if your sheep!"
But they were among the few who spoke up to echo Mr. Trump's refrain that he was being denied his due in the form of winning the election, a primal scream emanating from the president that was summed up earlier in the day by his own angry, plaintive, all-caps tweet: "STOP THE COUNT!"
Posted in Business, Leadership, U.S., Uncategorized and tagged Election, election fraud, Lindsey Graham, Trump. Bookmark the permalink.
Trump's Call to Halt Vote Counts is a Dangerous Attack on Democracy
China's "Iron Crotch" Masters Fight To Preserve Painful Tradition


We are so fortunate to be able to work with amazing brides as well as incredible venues! We thought it would be fun to show all of our readers where we are working this year. Below is a montage of all the different venues that we have already been to this year and the ones that we will be at before the year is over! If you are a bride still on the hunt for your perfect venue, be sure to check out these locations!


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Kemey.net ከመይ.ኔት
ScienceEcon
Issayas Tesfamariam
A conversation with Deborah Sanguineti
Would you tell us about yourself?
I was born in Kainji, Nigeria in 1967. My father was running a hospital there and my mother was a nurse. (Both are Italian.) We came to the United States in 1971. I currently live in New York. I am the executive director and curator of the U.S. collection of my grandmother's collection (Nenne Sanguineti Poggi). Together, with my father, Dr. Vincenzo Sanguineti, we promote, exhibit, and share the story of this remarkable woman.
What is your connection with Eritrea?
My connection to Eritrea is through my grandparents and my father. My grandfather, Tito Sanguineti, went to Eritrea in 1935 during the era of Fascism under Mussolini. He was a mineral engineer for Agip in Asmara. When the war broke out, he was rejected from entering the military so he continued to work for Agip, delivering oil from Somalia to Asmara. But at one point, unclear why, he was taken as a prisoner by the English and was brought to Addis Ababa.
Would you elaborate on that?
My grandfather was organizing the delivery of oil to the Italian troupes from Port Djibouti and Somalia to Asmara. When the British army broke through the Italian front and occupied Eritrea, my grandfather was arrested and sent to Addis Ababa to a concentration camp. He escaped by foot and other local means, and made his way back to Asmara. He told me the story of how he escaped - by hiding in the garbage that would be brought out every few days. My grandfather spoke very little of his war experience, but my father recalls him sharing that a local, native woman may have helped him escape.
Your last name resembles that of Sergent Sanguneti who was held as a hostage by Degiat (title) Bahta Hagos in Segeneiti in 1894? Any connection?
No, there is no relation to Sergeant Sanguineti.
On your grandmother?
My grandmother, Nenne Sanguineti Poggi, arrived in Eritrea in 1937. My father was born in Asmara in 1938. He attended the Liceo Ferdinando Martini.
My grandmother arrived in Eritrea, already an accomplished artist. She and Arturo Mezzedimi would become friends, and he would entrust her to interpret his visions of complimenting architecture with decorations, like her mosaics on the Agazien School in Asmara. He would also introduce her to the Emperor Haile Sellassie, who commissioned her for various public works, including The Enda Mariam Church.
My grandmother was a very prolific painter. She had numerous exhibitions and received awards while in Eritrea, of which I have the original articles. She was also a special envoy for the U.N. Those 30 years were her happiest. She fell in love with everything about Eritrea, which is obvious because it permeated her artwork until she passed in 2012 at 103!
My grandmother and I were extremely close. Maybe because I was the daughter she never had, and she was the mother I wish I had had. So, it was necessary for me to go to Eritrea to see her public works with my own eyes. I finally made the trip in October with an Italian tour group of architects and engineers. We flew from Milano to Asmara for a 10-day tour of the country. My grandmother's autobiography best describes how she felt about Eritrea. She fell in love with the people, landscape...all of it. You can see it in her drawings and paintings on her website at www.nennesanguinetipoggi.com
Did I mention her latest exhibit will be in New York City in March at a gallery in TriBeCa?
What was/is your impression of your visit to Eritrea? Was it your first visit?
I traveled with a group with the College of Engineers and Architects of Milano, in collaboration with The Academy of Fine Arts of Brera. Yes, it was my first visit to Eritrea.
The first two days were spent in Asmara. A contact of a friend of mine who works at the Asmara Heritage Project, was kind enough to take me around Asmara to see Nenne's works as well as the city. The first one I came across was at the Agazien School. At first, I was frozen by the image. Then I cried tears of joy and disbelief that these beautiful symbols were right there in front of me, with her signature in the right-hand corner. Our next stop was the Enda Mariam Church with its 7 panels. I didn't cry this time. Once was all I needed. But I was awestruck by the presence it held as you walked up to it, and by the vivacious colors! Absolutely beautiful! Our third stop was at the old Cotonificio Barattolo, with her painted panels gracing the entrance. The manager was still there and kind enough to give us a tour of what is now "Dolce Vita". Our final stop was her stunning mosaics in the Casciani Chapel at the cemetery looking over the city.
We walked the entire city those two days, visiting the historical buildings which make up this world heritage site. As an Italian, I could see the Italian influence left behind..."Little Rome". But I also saw a beautiful people of all all ages and all walks of life. I recall seeing a muslim teenage girl in traditional clothing, walking arm in arm with another teenage girl wearing jeans and no headdress. I got the impression that, no matter what your religion, you would not live separate lives.
Back with the group, we traveled to the charmimg city of Keren, where the women wore more color than in Asmara, of vibrant reds and deep purples. The livestock market with its camels and goats and men draped in white futas was such fun. And watching the people go about their business through the streets, happy and serene, couldn't be more polar opposite to what you would see on the sidewalks of New York City.
On the road to Massawa, I would just stare out the window, taking it all in as much as I physically and mentally could. Someone on the trip asked me what I was thinking about. I was thinking about three people: my grandfather, my father and my grandmother. I tried imagining my grandfather, a young man, with adventure in his blood, making the road from Asmara to Tessenei and back again. His epitaph reads "40 years in Africa". I thought about my father, born here, growing up here, finding adventures to be had with his friends within the mountains, and how much of this far off land he carries with him to this day as he continues to live his lovely life in Philadelphia. And I think about my grandmother...am I looking at something she may have seen too, driven to stop and pull out her sketchbook, or return the following day with her paints and easel? I finally felt like I was there with them, the four of us all together in this majestic landscape. It was powerful. It was necessary.
Massawa, the port city on the Red Sea, was fascinating but not easy to visit because it is a war-torn city from when the war ended in 1991. I have never seen a war-torn city in person. These beautiful Ottoman and Italian influenced buildings have been severely bombed...and some of them have people living inside. It was so hot that residents would put their cots outside their doors to sleep. The children might be sleeping while the mothers made the ceremonial coffee, in part with hopes of selling one to a passer-by. My wish would be to see a complete restoration of these buildings, not tear them down to rebuild. But I realize the expense that goes with that.
Our next stop was Disse of the Dahlak Islands. We arrived during a sandstorm, a very uncomfortable sandstorm, especially if you wear contact lenses. But we slept under the stars. I opted for no tent, just a cot. I have never seen a sky so filled with planets and constellations and shooting stars and a Milky Way you could probably walk on....and a half moon so bright and so low that it woke me up one of the nights. We ate what had been fished that day, and we washed our plates and glasses in the sea with the sand. There was no running water, no bathrooms, no electricity, just 15 people getting to know each other, telling jokes and sharing stories.
There are more details I could share of what I saw and what I did, but it was the overall "feel" of this ancient land that captivated me, so much so that I am already thinking of WHEN I will go back. Because when I left, a small part of me felt like I left my grandmother behind. And that is because I have. She is on the church, on the school, on the factory, and certainly on other places I have yet to discover. The most special feeling I walked away with was pride. When people learned that I was the granddaughter of the artist who created the panels of the Enda Mariam Church, I could feel the respect they had for her, some also amazed because they never knew who the artist was! She is a part of Asmara as Asmara was a part of her.
Thank you, Deborah.
A Conversation with Brown University Anthropologist, Prof. Lina Fruzzetti. Part II
A Conversation with Brown University Anthropologist, Prof. Lina Fruzzetti. Part I
"The Miracle of Massawa*" Revisited: A Conversation with Ted Pollard, grandson of Commande
© 2020 kemey.net


Creativity: "Just Like My Dad!"
Photography, like most forms of art, may be presented as is or with creative enhancement. Is it possibly to take a watercolor photo in-camera, without digital manipulation?
"How to pick the pixels into a peck of Perfection..."
While driving home after church one Sunday, a brilliant idea popped into my head.
"Why don't I turn-off the windshield wiper blades for a few moments, point the camera through the window, and snap as many photos as I feel that I can safely snap. Wouldn't it be great to create a watercolor photo in-camera, with real water refracting the light, instead of a digital darkroom retouch?"
At times, however, a nice digital-edit of one of The LORD's beautiful flowers can render a blue heart inside of a nice new logo.
The effect is subtle, but the impact is powerful.
Isn't it amazing what a burn-in tool can do on three little nodules to change the entire photo?
The photographer's eye can be developed, (pardon the pun,) by observing rather than simply looking.
Shallow DOF (aka depth-of-field, meaning the in-focus area,) can create great impact by drawing the viewer's eye to the part of the photograph that the photographer wishes to emphasize. In this photo the out-of-focus areas act as framing to create a cameo-effect.
At times subtle is neither needed nor wanted, when enjoying life through the creation of the digital whimsy of cleverly-manufactured photos that make the reader think.
The following example has been left, slightly-incomplete, for the purpose of training the observant eye. Can you see the mistake in editing? It could be a little difficult, due to the distraction of this up and coming actress, but it is in there.
Capturing fireworks photos is a difficult proposition at best.
Capturing fireworks, without a steady-hand, that is made steadier by a fence post, is nearly impossible.
This photo is a compilation/montage of three or four photographs to increase the drama, the intensity, and the effect of the subject, "Fireworks!"
Flowers as photographic subjects have long been as much a love as a skill of this photographer.
Finding a nearly-perfect bloom, bejeweled with raindrops after a recent shower, was indeed an exquisite treasure.
Finding that it had been captured in strong focus to the greatest effect was a rare "feather-in-the-cap."
Creating a mirror-image photo can add a bit of fun to the photographer's workday, but a caveat emptor must be stated.
Mirror-image creations are an acquired taste.
Mirror-images, like this sunset, are unique, sometimes fun, whimsical, and can have a great deal of WOW-effect. However, just as often, they can seem rather disturbing, depending on the personal preferences of the viewer.
Digital photography may not be as simple as using silver halide crystals on acetate (aka film,) but the investment of time and effort can return great dividends of Oooos and Ahs.


In 1951 Winford was searching for an idea for a book that would be "something different," when a chance meeting with a former female impersonator gave him the idea. He spent three years researching and contacting performers from all over the country. In his epilogue he recounts how difficult this was, as he was met with suspicion from many who feared being made the subject of ridicule and gossip. While many of the attitudes in his writing are outdated by today's standards, it is my impression that the project evolved into an earnest attempt to present this as a legitimate form of entertainment.
Yeah, But Did She Get His Autograph?


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Cygnus Mission Control Fire Alarm Clears NG-18 Launch for 24 Hours
Northrop Grumman was preparing to launch the penultimate Antares 230+ rocket from Wallops Island, Va., for the NG-18 mission to the International Space Station (ISS) at 5:50 a.m. EST (10:50 a.m. UTC). Sunday, November 1. 6; however, a fire alarm in the Cygnus Mission Control Center initially pushed the launch to 5:55 a.m. EST, the end of the window, before finally scrubbing the launch for the day.
Teams have prepared for a 24-hour refresher and will attempt to launch NG-18 again in a 5-minute window that opens at 5:27 a.m. EST (10:27 UTC) on Monday, November 7.
Antares will carry an Enhanced Cygnus spacecraft, named the SS Sally Ridein orbit for an Expedition 68 crew resupply mission. Cygnus will bring crew supplies, new science experiments and other payloads, including a new Nanoracks module, to the station before serving disposal device at the end of its mission for soiled clothing, used experiments, general work and living waste.
Overall, according to Northrop Grumman in an interview with NASASpaceflight, "It's going to be a pretty standard mission. There's a full science complement," said Steve Krein, vice president of civil and commercial space for Northrop Grumman.
Behind that, however, is an increase in the payload that Northrop Grumman was able to carry on this mission.
"So we were able to refine our propulsion modeling, both on the first and second stage, and remove some of the conservatism from our models," said Kurt Eberly, director of space launch programs at Northrop Grumman. "We offered an additional 70 kilograms, so we launched 8,050 kilograms on NG-12 through 17. And so for NG-18 and 19, we increased that to 8,120 kilograms."
This total mass includes the wet mass of Cygnus after it is loaded with its thrusters necessary for maneuvering in orbit.
NG-18 will be the first of eight additional cargo flights that have been ordered by NASA from Northrop Grumman to extend Cygnus' pre-existing Commercial Resupply Services 2 (CRS2) contract. In total, NASA ordered two more flights in 2020, including NG-18 and NG-19, followed by six more in March 2022.
The Cygnus spacecraft for this mission is named after astronaut Sally Ride, who was the first American woman in space. Ride flew on two Space Shuttle missions aboard the Challenger: STS-7 and STS-41G. Ride was also a member of the Rogers commission after the Challenger disaster in 1986.
Ride died in 2012 from pancreatic cancer.
"There's actually a flag that we fly, an American flag signed by the students and staff of Sally Ride Elementary School in Los Angeles, California. So we're extremely proud to be able to do this, to honor his legacy," Krein said.
Launch the campaign
The first stage of the Antares rocket was designed and built in Ukraine. The stage was designed by KB Yuzhnoye and is derived from the now retired Zenit rocket. The stage was later built by Yuzhmash in Dnipro, Ukraine.
The NG-18 mission patch. (Credit: Northrop Grumman)
The launcher uses two Energomash RD-181 engines which were built in Russia. The engines each run on RP-1 kerosene and liquid oxygen (LOX) and have independent thrust vectoring.
The RD-181 engines replaced the Aerojet Rocketdyne AJ-26 engines, which were retrofitted versions of the Soviet NK-33 engines built by Kuznetsov's design bureau. AJ-26 engines were used on the first four Antares flights.
The RD-181 engines and the Antares first stage were delivered to Northrop Grumman in Wallops in the fourth quarter of 2021. The NG-18 and -19 mission hardware was unaffected by the Russian invasion of Ukraine .
The Cygnus spacecraft itself is made up of two segments: the service module, which includes the propulsion and the two solar panels, and the pressurized cargo module. The pressurized cargo module was built by Thales Alenia Space in Italy, while the service module was built by Northrop Grumman.
After Cygnus arrived at Wallops, the two segments were mated together, creating the spacecraft as a whole. After that, the spacecraft was transported to another facility on Wallops Island where it was loaded with hydrazine and nitrogen tetroxide propellants. It was then reverted to the Horizontal Integration Facility (HIF).
The spacecraft was then brought into a horizontal position, allowing personnel to carry out an initial load of cargo. Cygnus was later incorporated into the Castor 30XL second stage. This was followed by another cargo before the fairing encapsulation.
The Antares 230+ rocket exits HIF for the 1.7 km journey to Pad-0A on November 2. (Credit: NASA)
On November 2, the Antares 230+ rocket deployed from HIF and was flown 1.7 km (1.1 miles) south to Pad-0A. Once on the launch pad, the vehicle rolled down the ramp and was integrated into the launch pad.
"We take that [Antares] up the ramp to the launch pad, we connect the tail to hydraulic pistons that are buried in a pit on the ramp, and then we push vertically," Eberly said.
The following day, the teams conducted a combined systems test, which verifies the interfaces between the vehicle, the launch pad and the NASA range.
Later in the day, Antares was lowered to a horizontal position and a mobile clean room was then moved above the nose of the rocket, allowing teams to perform late loading operations 24 hours before launch. .
"We have this unique feature that we've developed, which we call the 'pop-top' fairing, where we can remove the nose cone from the fairing. And that exposes the Cygnus hatch through the fairing opening. And then we set up work platforms on the surface of the fairing and then we can crawl the Cygnus cargo operators," Eberly said.
Once the late loading is complete, the "pop-top" fairing is reinstalled and the vehicle is brought upright for launch.
The countdown to the Nov. 6 launch began at 05:50 UTC or 1:50 a.m. EDT – 10 minutes before the local time change in Wallops to Eastern Standard Time (EST), which reset the local clock at 1:00 a.m. EST and therefore gave the launch team the full five hours needed for the Antares countdown.
The countdown to the November 7 launch will begin at 00:27 EST (05:27 UTC).
Journey to the ISS
At T0, the Antares rocket will take off from Pad-0A. The first stage RD-181 engines will burn for about two and a half minutes.
Cygnus is captured by Canadarm2 during the NG-17 mission in February 2022. (Credit: NASA)
Following this, the single Castor 30XL will ignite and burn for several minutes. The second stage is a solid rocket motor developed by Northrop Grumman. After burnout, the Cygnus spacecraft will separate into low Earth orbit, which will occur approximately nine minutes after launch.
"After separation, we do a few maneuvers with the upper stage just to make sure there's no recontact between us and Cygnus using our attitude control system," Eberly said. "So we're kind of doing a crab-walking maneuver to back up to make sure there's a good separation between us and Cygnus."
After separation, Cygnus will begin to perform periodic burns to enable it to make a timely rendezvous with the ISS. The two solar panels will begin to deploy approximately two hours after launch.
Cygnus is expected to arrive at the ISS two days after launch. NASA astronaut Nicole Mann will capture the spacecraft with Canadarm2 and then dock it at one of the Station's US segment ports.
The spacecraft is expected to remain at the ISS until January 2023.
Development Antares 330
After the launch of NG-18, the final launch of the Antares 230+ will take place in the spring of 2023 with the NG-19 mission. This comes as Northrop Grumman responds to the Russian invasion of Ukraine by developing a new version of Antares with Firefly Aerospace.
After NG-19, three Cygnus missions, NG-20, -21 and -22, will launch on SpaceX's Falcon 9 rocket during the interim period when Firefly and Northrop Grumman continue to develop the Antares 330.
"We want to resume these CRS missions as soon as possible. So the first increment is only the first stage which is just hard enough of course, but the Antares 330 is going to have the first stage supplied by Firefly, mated to the existing top stack. And so we think that just minimizes the range of Firefly, and it minimizes the development to allow us to resume CRS missions out of Virginia," Eberly said.
A render of the Antares 330. (Credit: Northrop Grumman)
The Antares 330 will consist of the same Castor 30XL upper stage that is currently used on Antares, but the first stage will be developed by Firefly Aerospace and will be similar to their Medium Launch Vehicle (MLV) rocket that is also in development. The first stage will be powered by seven Miranda engines.
"We are working very hard with Firefly on the development of this first stage which will form the basis of the Antares 330. And the employees we have here at Wallops, we intend to keep all of them. So we're putting them to work helping us grow this next stage and our employees in Dulles, VA, and Chandler, Arizona," Eberly said.
In addition, modifications will have to be made to the existing infrastructure on Wallops Island.
"We need to adjust the ground support equipment inside the HIF, we need to expand the carrier mount launcher, and then we're also working with Virginia Space to figure out what pad modifications we're going to need. for this new rocket configuration," Eberly said.
"It's going to have a lot more thrust, maybe have a little bit larger diameter, it's going to be longer. So all of those things are going to conspire to require us to add launchpad capability. And so that's also in preparation for.
The Antares 330 will also facilitate new modifications to upgrade the Cygnus spacecraft.
"On the Cygnus side, we have won the contract for the next six missions. And one of those add-ons is what we call a mission configuration B, which actually has an extra ring if you will, at the pressure containment module. Mission B configuration in the future will allow us to fly 5,000 kilograms of [cargo] mass," Krein said.
Along with the Antares 330, Northrop Grumman and Firefly Aerospace are developing a new launch vehicle that will be built entirely in the country and will be available for NASA, commercial and national security markets.
"We will then take that same first stage for the Antares 330, and then we will develop with Firefly a new liquid second stage with a larger fairing," Eberly said.
"We're calling it the mid-launch, and we're going to go through an internal naming contest with our people here…both us and Firefly. We'll see who wins. But this capability that we're targeting to debut at the end of 2025. We think it will be a really strong contender.
(Main image: The Antares 230+ spacecraft arrives at Pad-0A on November 2. Credit: NASA)


text:
Claudiu Iulian Niculescu (né le  à Slatina en Roumanie) est un footballeur international roumain devenu entraîneur.

Biographie

Palmarès

Comme joueur

Universitatea Craiova
 Finaliste de la Coupe de Roumanie en 1998 et 2000

Dinamo Bucarest
 Champion de Roumanie en 2002, 2004 et 2007
 Vainqueur de la Coupe de Roumanie en 2003, 2004 et 2005
 Vainqueur de la Supercoupe de Roumanie en 2005
 Meilleur buteur du Championnat de Roumanie en 2005 (21 buts) et 2007 (18 buts)

Comme entraîneur

FC Voluntari
 Vainqueur de la Coupe de Roumanie en 2017
 Vainqueur de la Supercoupe de Roumanie en 2017

Notes et références

Liens externes

Naissance à Slatina
Naissance en juin 1976
Footballeur international roumain
Joueur du FC Universitatea Craiova
Joueur du Dinamo Bucarest
Joueur du Genoa CFC
Joueur du MSV Duisbourg
Joueur de l'Omónia Nicosie
Joueur du CF Universitatea Cluj-Napoca
Entraîneur roumain de football


Welcome to Mr. Suave's Mod Mod World. This week's show is brought to you by the letter Y as in Y chromosome. It's mod men week on the modcast. I've collected songs from mod men, some with undeniable mod street cred like Ray Davies, Steve Marriot, or Paul Weller, and to others like Mose Allison and Paul Heaton who I will go to my grave arguing are every bit the mod as any other man. Regardless of all that, you can't argue with the songs. It's another great mix, if I do say so myself.
It was hard to put together the list, partly because what I really wanted were established artists who were now doing solo work. It was easy for some of them. Then there were others, like Steve Marriot who I really wanted to put in the show, that I had to dig deep and still found them in a band situation, or guys like Mose Allison who have essentially been solo artists for their entire careers, I included them anyhow.


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Description: Join us for food, fun and rides at our annual Summer Social.
Join us for our annual Ladies Salad Supper featuring Spring fashions and decor from Gehlhausens. Please bring a salad or a dessert to share.
Join us for food, fun and rides at our annual Summer Social.